Speaker
Description
Starburst regions in a galaxy are the primary source of stellar-driven winds, which contribute to regulating the star-formation cycle. We investigate the properties of the gas distribution, kinematics, and ionization conditions of the near-side outflow along eight sightlines that reside in the 30 Doradus region of the LMC using UV absorption-line and H I 21-cm radio emission-line observations. We find that within 0.52 degrees from the center of 30 Doradus, the wind reaches maximum speeds of 100-165 km/s from the LMC's disk. The total integrated column densities of low-ions in the blueshifted wind are highest near the center of this starburst region and decline radially outward. We estimate an outflow mass of M ~ (5.7-8.6) x 10^5 Mⵙ, outflow rate of (dM/dt) ≳0.02 Mⵙ/yr, and mass loading factor of ≳0.10 for this region. The observed ion ratios, together with photoionization modeling, reveal that this wind is roughly 40-97% photoionized. We also estimated the metallicities and dust depletion patterns of two of the high-velocity absorbers and found one being consistent with a LMC origin and the other with a MW. The high-ion lines are broader and exhibit kinematic offsets compared to the low-ions, indicating the presence of turbulent mixing layers within the wind. Finally, our hydrodynamical simulations of the Magellanic Clouds (MCs) and MW system suggest that the Magellanic Corona can protect the LMC winds from the ram-pressure forces exerted by the MW's halo.
